Low-mass stars in the Orion region

Details Low-mass stars in the Orion region Low-mass stars in the Orion region

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.135..237i&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 135, no. 2, July 1987, p. 237-244.

Astronomy and Astrophysics

Astrophysics

2

Interstellar Matter, Molecular Clouds, Orion Nebula, Star Formation Rate, Stellar Mass, Density Distribution, Stellar Mass Ejection, Stellar Radiation

Scientific paper

Recent observational evidence shows that low-mass stars were firstly formed in molecular clouds, and that, at a later stage when massive stars were formed, the formation rate of low-mass stars was still high in the Orion nebula (this paper) but decreases rapidly in NGC 2264 (Adams et al., 1983). This difference is probably caused by the effects of mass ejection and luminous radiation from the stars which were born in the previous period. In this paper, the author discusses examples of low-mass stars in order to find a relationship between the age and location of stars.

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